  We discovered Fe $K_{\alpha}$ complex emission and pulsation in two highly
variable sources (4XMM J174917.7--283329, 4XMM J174954.6--294336). The
equivalent widths of 6.4 and 6.7 keV lines of 4XMM J174917.7--283329 are
$99^{+84}_{-72}$ and $220^{+160}_{-140}$ eV, respectively. The continuum is
fitted by a partially absorbed apec model with plasma temperature of
$kT=13^{+10}_{-2}$ keV. The inferred mass of the white dwarf (WD) is
$0.9^{+0.3}_{-0.2}\ M_{\odot}$. We detected pulsations with a period of
$1212\pm3$ s and a pulsed fraction of $26\pm6\%$. The light curves of 4XMM
J174954.6--294336 display asymmetric eclipse and dipping behaviour. To date,
this is only the second intermediate polar (IP) that shows a total eclipse in
X-rays. The spectrum of the sources is characterized by a power-law model with
photon index $\Gamma=0.4\pm0.2$. The equivalent widths of the 6.4 keV and 6.7
keV iron lines are $171^{+99}_{-79}$ and $136^{+89}_{-81}$ eV, respectively.
The continuum is described by emission from optically thin plasma with a
temperature of $kT\sim35$ keV. The inferred mass of the WD is
$1.1^{+0.2}_{-0.3}\ M_{\odot}$. We discovered coherent pulsations from the
source with a period of $1002\pm2$ s. The pulsed fraction is $66\pm15\%$. The
measured spin period, hard photon index, and equivalent width of the
fluorescent Fe $K_{\alpha}$ line in both sources are consistent with the values
found in IP. While 4XMM J174954.6--294336 was already previously classified as
an IP, we also suggest 4XMM J174917.7--283329 as a new IP. The X-ray eclipses
in 4XMM J174954.6--294336 are most likely caused by a low-mass companion star
obscuring the central X-ray source. The asymmetry in the eclipse is likely
caused by a thick bulge that intercepts the line of sight during the ingress
phase but not during the egress phase located behind the WD along the line of
sight.
