  We construct the most complete sample of supernova remnants (SNRs) in any
galaxy - the Large Magellanic Cloud (LMC) SNR sample. We study their various
properties such as spectral index ($\alpha$), size and surface-brightness. We
suggest an association between the spatial distribution, environment density of
LMC SNRs and their tendency to be located around supergiant shells. We find
evidence that the 16 known type Ia LMC SNRs are expanding in a lower density
environment compared to the Core-Collapse (CC) type. The mean diameter of our
entire population (74) is 41 pc, which is comparable to nearby galaxies. We
didn't find any correlation between the type of SN explosion, ovality or age.
The $N(<D)$ relationship of $a={0.96}$ implies that the randomised diameters
are readily mimicking such an exponent. The rate of SNe occurring in the LMC is
estimated to be $\sim$1 per 200 yr. The mean $\alpha$ of the entire LMC SNR
population is $\alpha=-0.52$, which is typical of most SNRs. However, our
estimates show a clear flattening of the synchrotron $\alpha$ as the remnants
age. As predicted, our CC SNRs sample are significantly brighter radio emitters
than the type Ia remnants. We also estimate the $\Sigma - D$ relation for the
LMC to have a slope $\sim3.8$ which is comparable with other nearby galaxies.
We also find the residency time of electrons in the galaxy ($4.0-14.3$ Myr),
implying that SNRs should be the dominant mechanism for the production and
acceleration of CRs.
