  We perform a new analysis of the M dwarf-M dwarf eclipsing binary system NSVS
07394765 in order to investigate the reported hyper-inflated radius of one of
the component stars. Our analysis is based on archival photometry from the Wide
Angle Search for Planets (WASP), new photometry from the 32 cm {Command Module
Observatory (CMO) telescope in Arizona and the 70 cm telescope at Thacher
Observatory in California}, and new high-resolution infrared spectra obtained
with the Immersion Grating Infrared Spectrograph (IGRINS) on the Discovery
Channel Telescope. The masses and radii we measure for each component star
disagree with previously reported measurements. We show that both stars are
early M-type main-sequence stars without evidence for youth or hyper-inflation
($M_1= 0.661\ ^{+0.008}_{-0.036}\ \rm{M_{sun}}$, $M_2= 0.608\
^{+0.003}_{-0.028}\ \rm{M_{sun}}$, $R_1= 0.599\ ^{+0.032}_{-0.019}\
\rm{R_{sun}}$, $R_2= 0.625\ ^{+0.012}_{-0.027}\ \rm{R_{sun}}$), and we update
the orbital period and eclipse ephemerides for the system. We suggest that the
likely cause of the initial hyper-inflated result is the use of
moderate-resolution spectroscopy for precise radial velocity measurements.
