AR Scorpii1 appears to be an example. It is a binary system, consisting of a white dwarf and an M-type red dwarf. It was apparently originally classified as a $\delta$ Scuti variable star, but it was later discovered to be a true close binary, with a period of 3.56 hours.
The white dwarf emits pulses, as discovered by Marsh et al. (2016), with a period of about two minutes. These are visible in wavelengths from ultraviolet to radio (see Fig. 2):
The most noticeable patterns are in the ultraviolet, and the weakest are in the radio band, but the signals are certainly detectable.
The rational for determining that the compact object is a white dwarf follows from its luminosity, its relatively long spin period (longer than any neutron star pulsar yet discovered), and the fact that the pairing with a red dwarf is "more natural" than the odd alternative involving a low-mass neutron star and high-mass red dwarf.
The system may form what is known as an intermediate polar, involving accretion onto a white dwarf influenced by the object's strong magnetic field. The other notable example is AE Aquarii, as Rob Jeffries mentioned. However, its radio emissions do not involve pulsations. Why it doesn't emit pulsating signals at radio wavelengths is another question entirely, and not one I can answer right now.
More recent results (Buckley et al. (2017)) indicate that the radio emissions from the system are polarized, similar to those of neutron stars. It seems that AR Sco shares even more characteristics with pulsars than was previously thought.
1 The Wikipedia page, I just discovered, is terrible.