  (Abridged) We present a spatial and spectral X-ray analysis of the Galactic
supernova remnant (SNR) G352.7-0.1 using archival data from observations made
with XMM-Newton and Chandra. Prior X-ray observations of this SNR revealed a
thermal center-filled morphology which contrasts with a shell-like radio
morphology, thus establishing G352.7$-$0.1 as a mixed-morphology SNR (MMSNRs).
Our study confirms that the X-ray emission comes from the SNR interior and must
be ejecta-dominated. Spectra obtained with XMM-Newton may be fit satisfactorily
with a single thermal component (namely a non-equilibrium ionization component
with enhanced abundances of silicon and sulfur). In contrast, spectra extracted
by Chandra from certain regions of the SNR cannot always be fit by a single
thermal component. For those regions, a second thermal component with solar
abundances or two thermal components with different temperatures and thawed
silicon and sulfur abundances (respectively) can generate a
statistically-acceptable fit. We argue that the former scenario is more
physically-plausible: based on parameters of our spectral fits, we calculate
physical parameters including X-ray-emitting mass (about 45 solar masses, for
solar abundances). We find no evidence for overionization in the X-ray emitting
plasma associated with the SNR: this phenomenon has been seen in other MMSNRs.
We have conducted a search for a neutron star within the SNR using a hard (2-10
keV) Chandra image but could not identify a firm candidate. We also present
(for the first time) the detection of infrared emission from this SNR as
detected at 24 micron by MIPS aboard Spitzer. Finally, we discuss the
properties of G352.7-0.1 in the context of other ejecta-dominated MMSNRs.

High Energy Astrophysical Phenomena