  This work reports on the detection of $\gamma$-ray emission coincident with
the supernova remnant (SNR) SNR G5.7-0.1 using data collected by the Large Area
Telescope aboard the Fermi Gamma-ray Space Telescope. The SNR is believed to be
interacting with molecular clouds, based on 1720 MHz hydroxyl (OH) maser
emission observations in its direction. This interaction is expected to provide
targets for the production of $\gamma$-ray emission from $\pi^0$-decay. A
$\gamma$-ray source was observed in the direction of SNR G5.7-0.1, positioned
nearby the bright $\gamma$-ray source SNR W28. We model the emission from radio
to $\gamma$-ray energies using a one-zone model. Following consideration of
both $\pi^0$-decay and leptonically dominated emission scenarios for the
MeV-TeV source, we conclude that a considerable component of the $\gamma$-ray
emission must originate from the $\pi^0$-decay channel. Finally, constraints
were placed on the reported ambiguity of the SNR distance through X-ray column
density measurements made using XMM-Newton observations. We conclude SNR
G5.7-0.1 is a significant $\gamma$-ray source positioned at a distance of $\sim
3$ kpc with luminosity in the 0.1--100 GeV range of $L_{\gamma} \approx 7.4
\times 10^{34}$ erg/s.
