  This paper reports on the $\gamma$-ray properties of the 2018 Galactic nova
V392 Per, spanning photon energies $\sim$0.1 GeV to 100 TeV by combining
observations from the Fermi Gamma-ray Space Telescope and the HAWC Observatory.
In one of the most rapidly evolving $\gamma$-ray signals yet observed for a
nova, GeV $\gamma$ rays with a power law spectrum with index $\Gamma = 2.0 \pm
0.1$ were detected over eight days following V392 Per's optical maximum. HAWC
observations constrain the TeV $\gamma$-ray signal during this time and also
before and after. We observe no statistically significant evidence of TeV
$\gamma$-ray emission from V392 Per, but present flux limits. Tests of the
extension of the Fermi/LAT spectrum to energies above 5 TeV are disfavored by 2
standard deviations (95\%) or more. We fit V392 Per's GeV $\gamma$ rays with
hadronic acceleration models, incorporating optical observations, and compare
the calculations with HAWC limits.
