  We report the first XMM detection of the SNR candidate G337.2+0.1 (=AX
J1635.9-4719). The object shows centrally filled and diffuse X-ray emission.
The emission peaks in the hard 3.0-10.0 keV band. A spatially resolved spectral
study confirms that the column density of the central part of the SNR is about
N_{H}~5.9 +/- 1.5*10^{22} cm^{-2} and its X-ray spectrum is well represented by
a single power-law with a photon index Gamma=0.96 +/- 0.56. The non-detection
of line emission in the central spectrum is consistent with synchrotron
radiation from a population of relativistic electrons. Detailed spectral
analysis indicates that the outer region is highly absorbed and quite softer
than the inner region, with N_{H}~16.2(+/-5.2)*10^{22} cm^{-2} and
kT=4.4(+/-2.8) keV. Such characteristics are already observed in other X-ray
plerions. Based on the morphological and spectral X-ray information, we confirm
the SNR nature of G337.2+0.1, and suggest that the central region of the source
is a pulsar wind nebula (PWN), originated by an energetic though yet undetected
pulsar, that is currently losing energy at a rate of ~ 10^{36} erg s^{-1}.
