  When the accreting white dwarf in a magnetic cataclysmic variable star (mCV)
has a field strength in excess of 10 MG, it is expected to synchronize its
rotational frequency to the binary orbit frequency, particularly at small
binary separations, due to the steep radial dependence of the magnetic field.
We report the discovery of an mCV (SDSS J134441.83+204408.3; hereafter, J1344)
that defies this expectation by displaying asynchronous rotation
($P_{spin}/P_{orb} = 0.893$) in spite of a high surface field strength (B=56
MG) and a short orbital period (114 min). Previously misidentified as a
synchronously rotating mCV, J1344 was observed by TESS during sector 50, and
the resulting power spectrum shows distinct spin and orbital frequencies, along
with various sidebands and harmonics. Although there are several other
asynchronous mCVs at short orbital periods, the presence of cyclotron humps in
J1344's SDSS spectrum makes it possible to directly measure the field strength
in the cyclotron-emitting region; a previously study estimated 65 MG based on
its identification of two cyclotron humps, but we revise this to 56$\pm$2 MG
based on the detection of a third hump and on our modeling of the cyclotron
spectrum. Short-period mCVs with field strengths above 10 MG are normally
expected to be synchronous, so the highly asynchronous rotation in J1344
presents an interesting challenge for theoretical studies of spin-period
evolution.
