  In the first months after the launch in July 2019, eROSITA onboard Spektr-RG
(SRG) performed long-exposure observations in the regions around SN 1987A and
SNR N132D in the Large Magellanic Cloud (LMC). We analyse the distribution and
the spectrum of the diffuse X-ray emission in the observed fields to determine
the physical properties of the hot phase of the interstellar medium (ISM). The
eROSITA data are complemented by newly derived column density maps for the
Milky Way and the LMC, 888 MHz radio continuum map from the Australian Square
Kilometer Array Pathfinder (ASKAP), and optical images of the Magellanic Cloud
Emission Line Survey (MCELS). We detect significant emission from thermal
plasma with kT=0.2 keV in all the regions. There is also an additional
higher-temperature emission component from a plasma with kT = 0.7 keV. In
addition, non-thermal X-ray emission is significantly detected in the
superbubble 30 Dor C. The absorbing column density NH in the LMC derived from
the analysis of the X-ray spectra taken with eROSITA is consistent with the NH
obtained from the emission of the cold medium over the entire area. Neon
abundance is enhanced in the regions in and around 30 Dor and SN 1987A,
indicating that the ISM has been chemically enriched by the young stellar
population. Emission from the stellar cluster RMC 136 and the Wolf-Rayet stars
RMC 139 and RMC 140 is best modelled with a high-temperature (kT>1 keV)
non-equilibrium ionisation plasma emission and a non-thermal component with a
photon index of {\Gamma} =1.3. In addition, the optical SNR candidate
J0529-7004 is also detected with eROSITA and we thus confirm the source as an
SNR.
