I think the main reason the answer doesn't come out correct is that the simple Hubble's law equation:
$v = dH_{0}$
Is only applicable in the local universe (Hence $H_{0}$, the value of the Hubble constant today). The rate of expansion of the Universe (the Hubble parameter) is determined by the composition of its energy density. Today, the composition is about 30% matter and 70% dark energy. In the recent past the energy density was dominated by matter. In the more distant past the energy density was dominated by relativistic particles (photons and neutrinos). The rate of expansion of the universe is different in each of these "epochs". In general the universe used to expand more rapidly (expansion has slowed thanks to the effects of matter), but distances also used to be smaller (the universe itself was smaller). Combine all of this together and you have a very complicated relationship between distance and the recessional velocity we observe today. This relationship does not have a simple functional form.
I think the easiest question to ask is: "How far has a photon traveled such that if it were emitted at the beginning of the universe it would reach me today?". The answer to this question is the "cosmological horizon", which we commonly talk about as being the size of the observable universe. To answer this question you need to use the spacetime metric which applies for our universe (Called the Friedmann-Robertson-Walker-Lemaitre metric). This is basically the relationship between speed, time, and distance in the realm of general relativity. If our universe is flat (which we think it must be) this equation is actually quite simple, but unfortunately it requires that you know how the universe has been expanding over its lifetime. As I mentioned this relationship has no closed form equation or number, which is why you will never see a simple equation for the solution you are looking for. You need to integrate the solution numerically. Wikipedia has a good little article on the horizon.
If you're interested, you'd write down the FLRW metric for a photon travelling in a "straight path":
$ cdt = \frac{a(t) dr}{ \sqrt{1-kr^2} } $
Where $a(t)$ is the scale factor of the universe, which tells you about its expansion history. This is the complicated function. $k$ is the curvature constant, which for a flat universe is 0. You then get:
$ \int^{t_{0}}_{0} \frac{c dt}{a(t)} = \int^{r_{H}}_{0} dr = r_{H} $
Here $t_{0}$ is the age of the universe and $r_{H}$ is the particle horizon you're interested in. To figure out $a(t)$ you need the Friedmann equations, which are functions of the different energy densities (dark energy, matter, relativistic particles, curvature), and the rates at which they change in time. I used astropy to do the integration and got $\approx 3.35 c t_{0}$ which gives about 14 Mpc, so close enough to the answer that you could attribute any differences to a difference in measured parameters that go into solving the integral.
I'd recommend Introduction to Cosmology by Ryden as a textbook if you really want to get into it.
