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We present ALMA (0.87~mm and 1.3~mm) and VLA (9~mm) observations toward thecandidate intermediate-mass protostar OMC2-FIR3 (HOPS-370;L$_{bol}$~314~L$_{\odot}$) at $\sim$0.1" (40~au) resolution for the continuumemission and ~0.25" (100 au) resolution of nine molecular lines. The dustcontinuum observed with ALMA at 0.87~mm and 1.3~mm resolve a near edge-on disktoward HOPS-370 with an apparent radius of ~100 au. The VLA observations detectboth the disk in dust continuum and free-free emission extended along the jetdirection. The ALMA observations of molecular lines (H$_2$CO, SO, CH$_3$OH,$^{13}$CO, C$^{18}$O, NS, and H$^{13}$CN) reveal rotation of the apparent disksurrounding HOPS-370 orthogonal to the jet/outflow direction. We fit radiativetransfer models to both the dust continuum structure of the disk and molecularline kinematics of the inner envelope and disk for the H$_2$CO, CH$_3$OH, NS,and SO lines. The central protostar mass is determined to be $\sim$2.5 M_sunwith a disk radius of $\sim$94~au, when fit using combinations of the H$_2$CO,CH$_3$OH, NS, and SO lines, consistent with an intermediate-mass protostar.Modeling of the dust continuum and spectral energy distribution (SED) yields adisk mass of 0.035~M$_{\odot}$ (inferred dust+gas) and a dust disk radius of62~au, thus the dust disk may have a smaller radius than the gas disk, similarto Class II disks. In order to explain the observed luminosity with themeasured protostar mass, HOPS-370 must be accreting at a rate between 1.7 and3.2$\times$10$^{-5}$~M$_{\odot}$~yr$^{-1}$.

astrophysical journal/the astrophysical journal

The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion  Protostars IV. Unveiling the Embedded Intermediate-Mass Protostar and Disk  within OMC2-FIR3/HOPS-370