  Large-amplitude accretion outbursts in young stars are expected to play a
central role in proto-stellar assembly. Outburst identification historically
has taken place using optical techniques, but recent, systematic infrared
searches are enabling their discovery in heavily dust-obscured regions of the
Galactic plane. Here, we present the discovery of WTP$\,$10aaauow, a
large-amplitude mid-infrared (MIR) outburst identified in a systematic search
of NEOWISE data using new image subtraction techniques. The source is located
towards the RCW$\,$49 star-forming region, and estimated to be at a distance of
$\approx 4\,$kpc via Gaia parallax measurement. Concurrent with the MIR
brightening, the source underwent a $\gtrsim5\,$mag outburst in the optical and
near-infrared (NIR) bands, reaching a peak luminosity of
$\approx260\,$L$_\odot$ in 2014-2015, followed by a slow decline over the next
7 years. Analysis of the pre- and post-outburst spectral energy distributions
reveal a pre-outburst stellar photosphere at a temperature of $3600-4000\,$K,
surrounded by a likely two-component dust structure similar to a flat-spectrum
or Class I type YSO. We present optical and NIR spectroscopy that show a
GK-type spectrum in the optical bands exhibiting complex line profiles in
strong absorption features, and evidence for a wind reaching a terminal
velocity of $\approx 400\,$km$\,$s$^{-1}$. The NIR bands are characterized by a
cooler M-type spectrum exhibiting a forest of atomic and molecular features.
All together, the spectra demonstrate that WTP$\,$10aaauow is an FU Ori type
outburst. Ongoing systematic infrared searches will continue to reveal the
extent of this population in the Galactic disk.
