  We present ALMA (0.87~mm and 1.3~mm) and VLA (9~mm) observations toward the
candidate intermediate-mass protostar OMC2-FIR3 (HOPS-370;
L$_{bol}$~314~L$_{\odot}$) at $\sim$0.1" (40~au) resolution for the continuum
emission and ~0.25" (100 au) resolution of nine molecular lines. The dust
continuum observed with ALMA at 0.87~mm and 1.3~mm resolve a near edge-on disk
toward HOPS-370 with an apparent radius of ~100 au. The VLA observations detect
both the disk in dust continuum and free-free emission extended along the jet
direction. The ALMA observations of molecular lines (H$_2$CO, SO, CH$_3$OH,
$^{13}$CO, C$^{18}$O, NS, and H$^{13}$CN) reveal rotation of the apparent disk
surrounding HOPS-370 orthogonal to the jet/outflow direction. We fit radiative
transfer models to both the dust continuum structure of the disk and molecular
line kinematics of the inner envelope and disk for the H$_2$CO, CH$_3$OH, NS,
and SO lines. The central protostar mass is determined to be $\sim$2.5 M_sun
with a disk radius of $\sim$94~au, when fit using combinations of the H$_2$CO,
CH$_3$OH, NS, and SO lines, consistent with an intermediate-mass protostar.
Modeling of the dust continuum and spectral energy distribution (SED) yields a
disk mass of 0.035~M$_{\odot}$ (inferred dust+gas) and a dust disk radius of
62~au, thus the dust disk may have a smaller radius than the gas disk, similar
to Class II disks. In order to explain the observed luminosity with the
measured protostar mass, HOPS-370 must be accreting at a rate between 1.7 and
3.2$\times$10$^{-5}$~M$_{\odot}$~yr$^{-1}$.
