  We report the second extragalactic pulsar wind nebula (PWN) to be detected in
the MeV-GeV band by the Fermi-LAT, located within the Large Magellanic Cloud
(LMC). The only other known PWN to emit in the Fermi band outside of the Milky
Way Galaxy is N 157B which lies to the west of the newly detected gamma-ray
emission at an angular distance of 4 degrees. Faint, point-like gamma-ray
emission is discovered at the location of the composite supernova remnant (SNR)
B0453-685 with a ~ 4 sigma significance from energies 300 MeV - 2 TeV. We
present the Fermi-LAT data analysis of the new gamma-ray source, coupled with a
detailed multi-wavelength investigation to understand the nature of the
observed emission. Combining the observed characteristics of the SNR and the
physical implications from broadband modeling, we argue it is unlikely the SNR
is responsible for the gamma-ray emission. While the gamma-ray emission is too
faint for a pulsation search, we try to distinguish between any pulsar and PWN
component of SNR B0453-685 that would be responsible for the observed gamma-ray
emission using semi-analytic models. We determine the most likely scenario is
that the old PWN (t ~ 14,000 years) within B0453-685 has been impacted by the
return of the SNR reverse shock with a possible substantial pulsar component
below 5 GeV.
