  The heart of the Large Magellanic Cloud, 30 Doradus, is a complex region with
a clear core-halo structure. Feedback from the stellar cluster R$\,$136 has
been shown to be the main source of energy creating multiple pc-scale
expanding-shells in the outer region, and carving a nebula core in the
proximity of the ionization source. We present the morphology and strength of
the magnetic fields (B-fields) of 30 Doradus inferred from the far-infrared
polarimetric observations by SOFIA/HAWC+ at 89, 154, and 214$\,\mu$m. The
B-field morphology is complex, showing bending structures around R$\,$136. In
addition, we use high spectral and angular resolution [\textsc{CII}]
observations from SOFIA/GREAT and CO(2-1) from APEX. The kinematic structure of
the region correlates with the B-field morphology and shows evidence of
multiple expanding shells. Our B-field strength maps, estimated using the
Davis-Chandrasekhar-Fermi method and structure-function, show variations across
the cloud within a maximum of 600, 450, and 350$\,\mu$G at 89, 154, and
214$\,\mu$m, respectively. We estimated that the majority of the 30 Doradus
clouds are sub-critical and sub-Alfv\'enic. The probability distribution
function of the gas density shows that the turbulence is mainly compressively
driven, while the plasma beta parameter indicates supersonic turbulence. We
show that the B-field is sufficient to hold the cloud structure integrity under
feedback from R$\,$136. We suggest that supersonic compressive turbulence
enables the local gravitational collapse and triggers a new generation of stars
to form. The velocity gradient technique (VGT) using [\textsc{CII}] and CO(2-1)
is likely to confirm these results.
