  We present a study of the supernova remnant MCSNR J0512-6707 in the Large
Magellanic Cloud. We used new data from XMM-Newton to characterise the X-ray
emission and data from the Australian Telescope Compact Array, the Magellanic
Cloud Emission Line Survey, and Spitzer to gain a picture of the environment
into which the remnant is expanding. We performed a morphological study,
determined radio polarisation and magnetic field orientation, and performed an
X-ray spectral analysis. We estimated the its size to be 24.9 (\pm1.5) x 21.9
(\pm1.5) pc, with the major axis rotated ~29 deg east of north. Radio
polarisation at 3 cm and 6 cm indicate a higher degree of polarisation in the
NW and SE tangentially oriented to the SNR shock front, indicative of an SNR
compressing the magnetic field threading the interstellar medium. The X-ray
spectrum is unusual as it requires a soft (~0.2 keV) CIE thermal plasma of
interstellar medium abundance, in addition to a harder component. Using our
results and the Sedov dynamical model, we showed that this emission is not
consistent with a Sedov remnant. We suggested that the thermal X-rays can be
explained by MCSNR J0512-6707 having initially evolved into a wind-blown cavity
and is now interacting with the surrounding dense shell. The origin of the hard
component remains unclear. We could not determine the supernova type from the
X-ray spectrum. Indirect evidence was found in the study of the local stellar
population and star formation history in the literature, which suggests a
core-collapse origin. MCSNR J0512-6707 likely resulted from the core-collapse
of high mass progenitor which carved a low density cavity into its surrounding
medium, with the soft X-rays resulting from the impact of the blast wave with
the surrounding shell. The unusual hard X-ray component requires deeper and
higher spatial resolution radio and X-ray observations to confirm its origin.
