  We present the characterization of CRTS J055255.7$-$004426 (=THOR 42), a
young eclipsing binary comprising two pre-main sequence M dwarfs (combined
spectral type M3.5). This nearby (103 pc), short-period (0.859 d) system was
recently proposed as a member of the $\sim$24 Myr-old 32 Orionis Moving Group.
Using ground- and space-based photometry in combination with medium- and
high-resolution spectroscopy, we model the light and radial velocity curves to
derive precise system parameters. The resulting component masses and radii are
$0.497\pm0.005$ and $0.205\pm0.002$ $\rm{M}_{\odot}$, and $0.659\pm0.003$ and
$0.424\pm0.002$ $\rm{R}_{\odot}$, respectively. With mass and radius
uncertainties of $\sim$1 per cent and $\sim$0.5 per cent, respectively, THOR 42
is one of the most precisely characterized pre-main sequence eclipsing binaries
known. Its systemic velocity, parallax, proper motion, colour-magnitude diagram
placement and enlarged radii are all consistent with membership in the 32 Ori
Group. The system provides a unique opportunity to test pre-main sequence
evolutionary models at an age and mass range not well constrained by
observation. From the radius and mass measurements we derive ages of 22-26 Myr
using standard (non-magnetic) models, in excellent agreement with the age of
the group. However, none of the models can simultaneously reproduce the
observed mass, radius, temperature and luminosity of the coeval components. In
particular, their H-R diagram ages are 2-4 times younger and we infer masses
$\sim$50 per cent smaller than the dynamical values.
