  We present the discovery and timing of the young (age $\sim 28.6$ kyr) pulsar
PSR J0837$-$2454. Based on its high latitude ($b = 9.8^{\circ}$) and dispersion
measure (DM $ = 143$~pc~cm$^{-3}$), the pulsar appears to be at a $z$-height of
$>$1 kpc above the Galactic plane, but near the edge of our Galaxy. This is
many times the observed scale height of the canonical pulsar population, which
suggests this pulsar may have been born far out of the plane. If accurate, the
young age and high $z$-height imply that this is the first pulsar known to be
born from a runaway O/B star. In follow-up imaging with the Australia Telescope
Compact Array (ATCA), we detect the pulsar with a flux density $S_{1400} = 0.18
\pm 0.05$ mJy. We do not detect an obvious supernova remnant around the pulsar
in our ATCA data, but we detect a co-located, low-surface-brightness region of
$\sim$1.5$^\circ$ extent in archival Galactic and Extragalactic All-sky MWA
Survey data. We also detect co-located H$\alpha$ emission from the Southern
H$\alpha$ Sky Survey Atlas. Distance estimates based on these two detections
come out to $\sim$0.9 kpc and $\sim$0.2 kpc respectively, both of which are
much smaller than the distance predicted by the NE2001 model ($6.3$ kpc) and
YMW model ($>25$ kpc) and place the pulsar much closer to the plane of the
Galaxy. If the pulsar/remnant association holds, this result also highlights
the inherent difficulty in the classification of transients as "Galactic"
(pulsar) or "extragalactic" (fast radio burst) toward the Galactic anti-center
based solely on the modeled Galactic electron contribution to a detection.
