  Aims. We present a multi-wavelength analysis of the evolved supernova
remnants MCSNR J0506-7025 and MCSNR J0527-7104 in the Large Magellanic Cloud.
Methods. We used data from XMM-Newton, the Australian Telescope Compact Array,
and the Magellanic Cloud Emission Line Survey to study their broadband emission
and used Spitzer and HI data to gain a picture of their environments. We
performed a multi-wavelength morphological study and detailed radio and X-ray
spectral analyses to determine their physical characteristics. Results. Both
remnants were found to have bright X-ray cores, dominated by Fe L-shell
emission, consistent with reverse shock heated ejecta with determined Fe masses
in agreement with Type Ia explosion yields. A soft X-ray shell, consistent with
swept-up interstellar medium, was observed in MCSNR J0506-7025, suggestive of a
remnant in the Sedov phase. Using the spectral fit results and the Sedov
self-similar solution, we estimated the age of MCSNR J0506-7025 to be ~16-28
kyr, with an initial explosion energy of (0.07-0.84)x10^51 erg. A soft shell
was absent in MCSNR J0527-7104, with only ejecta emission visible in an
extremely elongated morphology extending beyond the optical shell. We suggest
that the blast wave has broken out into a low density cavity, allowing the
shock heated ejecta to escape. We found that the radio spectral index of MCSNR
J0506-7025 is consistent with the standard ~0.5 for SNRs. Radio polarisation at
6 cm indicates a higher degree of polarisation along the western front and at
the eastern knot, with a mean fractional polarisation across the remnant of
P~(20 \pm 6)%. Conclusions. The detection of Fe-rich ejecta in the remnants
suggests that both resulted from Type Ia explosions. The newly identified
Fe-rich cores in MCSNR J0506-7025 and MCSNR J0527-7104 makes them members of
the expanding class of evolved Fe-rich remnants in the Magellanic Clouds.
