  We present ALMA band 6/7 (1.3 mm/0.87 mm) and VLA Ka band (9 mm) observations
toward NGC 2071 IR, an intermediate-mass star forming region. We characterize
the continuum and associated molecular line emission towards the most luminous
protostars, i.e., IRS1 and IRS3, on ~100 au (0. 2") scales. IRS1 is partly
resolved in millimeter and centimeter continuum, which shows a potential disk.
IRS3 has a well resolved disk appearance in millimeter continuum and is further
resolved into a close binary system separated by ~40 au at 9 mm. Both sources
exhibit clear velocity gradients across their disk major axes in multiple
spectral lines including C18O, H2CO, SO, SO2, and complex organic molecules
like CH3OH, 13CH3OH and CH3OCHO. We use an analytic method to fit the Keplerian
rotation of the disks, and give constraints on physical parameters with a MCMC
routine. The IRS3 binary system is estimated to have a total mass of
1.4-1.5$M_\odot$. IRS1 has a central mass of 3-5$M_\odot$ based on both
kinematic modeling and its spectral energy distribution, assuming that it is
dominated by a single protostar. For both IRS1 and IRS3, the inferred ejection
directions from different tracers, including radio jet, water maser, molecular
outflow, and H2 emission, are not always consistent, and for IRS1, these can be
misaligned by ~50$^{\circ}$. IRS3 is better explained by a single precessing
jet. A similar mechanism may be present in IRS1 as well but an unresolved
multiple system in IRS1 is also possible.
