  We present moderately deep (125 ks) {\it XMM-Newton} observations of
supernova remnant G330.2$+$1.0. This remnant is one of only a few known that
fall into "synchrotron-dominated" category, with the emission almost entirely
dominated by a nonthermal continuum. Previous X-ray observations could only
characterize the spectra of a few regions. Here, we examine the spectra from
fourteen regions surrounding the entire rim, finding that the spectral
properties of the nonthermal emission do not vary significantly in any
systematic way from one part of the forward shock to another, unlike several
other remnants of this class. We confirm earlier findings that the power-law
index, $\Gamma$, ranges from about 2.1-2.5, while the absorbing column density
is generally between 2.0-2.6 $\times 10^{22}$ cm$^{-2}$. Fits with the {\it
srcut} model find values of the roll-off frequency in the range of 10$^{17.1} -
10^{17.5}$ Hz, implying energies of accelerated electrons of $\sim 100$ TeV.
These values imply a high shock velocity of $\sim 4600$ km s$^{-1}$, favoring a
young age of the remnant. Diffuse emission from the interior is nonthermal in
origin as well, and fits to these regions yield similar values to those along
the rim, also implying a young age. Thermal emission is present in the east,
and the spectrum is consistent with a $\sim 650$ km s$^{-1}$ shock wave
encountering interstellar or circumstellar material with a density of $\sim 1$
cm$^{-3}$.
