According to Herczeg & Hillenbrand (2014) the intrinsic bolometric luminosity of T Tau is about $7L_\odot$ (for an assumed distance of 479 light years).
The main difference between their estimate and yours is that they have: (i) Taken account of extinction towards the object, which considerably dims its visible flux by about 1.25 magnitudes (a factor of 3.2). (ii) Taken account of the spectral energy distribution, which differs from the Sun.
You cannot in general calculate a ratio of luminosities from a difference in visual magnitudes, unless the spectral energy distributions of the two sources are the same. T Tau has a greater proportion of its flux emerging at near infrared wavelengths than the Sun.
T Tau is in a multiple system with a much lower mass companion (which contributes little to the luminosity), but this has led to a quite accurate mass determination of $(2.12 \pm 0.10)\ M_\odot$ (Kohler et al. 2015).
Given a main-sequence mass-luminosity trend of around $L \sim M^3$, then it is apparent that T Tau has around the luminosity it would be expected to have on the main sequence.
This would suggest that it has finished descending its Hayashi track in the HR diagram and is currently traversing, roughly horizontally, towards hotter temperatures and slightly rising luminosity, in excellent accordance with stellar evolutionary models (see below) if its age is $\sim 2$ Myr.
T Tau is only unsusual compared with most "T-Tauri stars" in that it has quite a high mass. Most "T-Tauri stars" are a solar mass or lower, and if found in young stellar clusters and associations with ages $<10$ Myr, you can see from the plot below that they would have higher luminosities than they end up with on the main sequence.
Pre main sequence evolutionary tracks and isochrones from Steven W. Stahler and Francesco Palla, "The Formation of Stars"; doi:10.1002/9783527618675