  We present Karl G. Jansky Very Large Array observations covering the NGC 1977
region at 3.0, 6.4, and 15.0 GHz. We search for compact radio sources and
detect continuum emission from 34 NGC 1977 cluster members and 37 background
objects. Of the 34 radio-detected cluster members, 3 are associated with known
proplyds in NGC 1977, 22 are associated with additional young stellar objects
in NGC 1977, and 9 are newly-identified cluster members. We examine the radio
spectral energy distributions, circular polarization, and variability of the
detected NGC 1977 sources, and identify 10 new candidate proplyds whose radio
fluxes are dominated by optically thin free-free emission. We use measurements
of free-free emission to calculate the mass-loss rates of known proplyds and
new candidate proplyds in NGC 1977, and find values $\sim10^{-9}-10^{-8}$
M$_{\odot}$ yr$^{-1}$, which are lower than the mass-loss rates measured
towards proplyds in the Orion Nebula Cluster, but consistent with the mass-loss
rates predicted by external photoevaporation models for spatially-extended
disks that are irradiated by the typical external UV fields encountered in NGC
1977. Finally, we show that photoevaporative disk winds in NGC 1977 may be
illuminated by internal or external sources of ionization, depending on their
positions within the cluster. This study provides new constraints on disk
properties in a clustered star-forming region with a weaker UV environment than
the Orion Nebula Cluster, but a stronger UV environment than low-mass
star-forming regions like Taurus. Such intermediate UV environments represent
the typical conditions of Galactic star and planet formation.
