  For the past decade, it has been suggested that intermediate polars (IPs), a
subclass of magnetic cataclysmic variables (CVs), are one of the main
contributors to the hard diffuse X-ray emission from the Galactic center (GC)
and Galactic ridge. In our ongoing \emph{XMM-Newton} survey of the central
region of the Galactic disk ($20^\circ\times2^\circ$), we detected a persistent
IP candidate, $1.7^\circ$ away from the GC. In this work, we better
characterize the behavior of this source by looking at the new and archival
XMM-Newton data. We performed a detailed X-ray spectral modeling of the source.
Furthermore, we searched for X-ray pulsations in the light curve as well as its
counterpart at other wavelengths. The XMM-Newton spectrum (0.8--10 keV) of the
source is described by a partial covering collisionally ionized diffuse gas
with plasma temperature $kT=15.7^{+20.9}_{-3.6}$ keV. In addition, the spectrum
shows the presence of iron lines at $E=6.44$, 6.65, and 6.92 keV with
equivalent widths of $194^{+89}_{-70}$, $115^{+79}_{-75}$, and $98^{+93}_{-74}$
eV, respectively. The X-ray light curve shows a coherent modulation with a
period of $P=432.44\pm0.36$ s, which we infer is the spin period of the white
dwarf. The white dwarf mass estimated from fitting a physical model to the
spectrum results in $M_{\rm WD}=1.05^{+0.16}_{-0.21}\ M_{\odot}$. We were able
to find a likely optical counterpart in the Gaia catalog with a G magnitude of
19.26, and the distance to the source derived from the measured Gaia parallax
is $\sim$4.3 kpc. We provide an improved source localization with subarcsec
accuracy. The spectral modeling of the source indicates the presence of
intervening circumstellar gas, which absorbs the soft X-ray photons. The
measured equivalent width of the iron lines and the detection of the spin
period in the light curve are consistent with those from IPs.
