  We present the results of a photometric and spectroscopic analysis of the
Galactic Bulge Survey X-ray source CXOGBS J174954.5-294335 (hereafter, referred
to as CX19). CX19 is a long period, eclipsing intermediate polar type
cataclysmic variable with broad, single-peaked Balmer and Paschen emission
lines along with HeII $\lambda4686$ and Bowen blend emission features. With
coverage of one full and two partial eclipses and archival photometry, we
determine the ephemeris for CX19 to be HJD(eclipse) = 2455691.8581(5) +
0.358704(2)$\times$N. We also recovered the white dwarf spin period of P$_{\rm
spin}$ = 503.32(3) seconds which gives a P$_{\rm spin}$/P$_{\rm orb}$ =
0.016(6), comparable to several confirmed, long period intermediate polars.
CX19 also shows a clear X-ray eclipse in the 0.3-8.0 keV range observed with
Chandra. Two optical outbursts were observed lasting between 6-8 hours (lower
limits) reaching $\sim$1.3 mags in amplitude. The outbursts, both in duration
and magnitude, the accretion disc dominated spectra and hard X-ray emission are
reminiscent of the intermediate polar V1223 Sgr sharing many of the same
characteristics. If we assume a main sequence companion, we estimate the donor
to be an early G-type star and find a minimum distance of $d \approx$ 2.1 kpc
and a 0.5-10.0 keV X-ray luminosity upper limit of 2.0 $\times$ 10$^{33}$ erg
s$^{-1}$. Such an X-ray luminosity is consistent with a white dwarf accretor in
a magnetic cataclysmic variable system. To date, CX19 is only the second
deeply-eclipsing intermediate polar with X-ray eclipses and the first which is
optically accessible.
