  We present a detailed analysis of SN 2020qmp, a nearby type IIP core-collapse
supernova (CCSN), discovered by the Palomar Gattini-IR (PGIR) survey in the
galaxy UGC07125. We illustrate how the multiwavelength study of this event
helps our general understanding of stellar progenitors and circumstellar medium
(CSM) interactions in CCSNe. We also highlight the importance of near-infrared
(NIR) surveys for early detections of SNe in dusty environments. SN 2020qmp
displays characteristic hydrogen lines in its optical spectra, as well as a
plateau in its optical LC, hallmarks of a type IIP SN. We do not detect linear
polarization during the plateau phase, with a 3 sigma upper limit of 0.78%.
Through hydrodynamical LC modeling and an analysis of its nebular spectra, we
estimate a progenitor mass of around 11 solar masses, and an explosion energy
of around 0.8e51 erg. We find that the spectral energy distribution cannot be
explained by a simple CSM interaction model, assuming a constant shock velocity
and steady mass-loss rate, and the excess X-ray luminosity compared with the
synchrotron radio luminosity suggests deviations from equipartition. Finally,
we demonstrate the advantages of NIR surveys over optical surveys for the
detection of dust-obscured CCSNe in the local universe. Specifically, our
simulations show that the Wide-Field Infrared Transient Explorer will detect
about 14 more CCSNe out of 75 expected in its footprint within 40 Mpc, over
five years than an optical survey equivalent to the Zwicky Transient Facility
would detect. We have determined or constrained the main properties of SN
2020qmp and of its progenitor, highlighting the value of multiwavelength
follow-up observations of nearby CCSNe. We have also shown that forthcoming NIR
surveys will finally enable us to do a nearly complete census of CCSNe in the
local universe.
