Based on an analysis of the interstellar highly ionized species Civ, Siiv, Nv and Ovi observed in the Far Ultraviolet Spectroscopic Explorer (FUSE) and Hubble Space Telescope/Space Telescope Imaging Spectrograph (HST/STIS) E140M spectra of four hot stars in the Large Magellanic Cloud (LMC), we find evidence for a hot LMC halo fed by energetic outflows from the LMC disc and even possibly an LMC galactic wind. Signatures for such outflows are the intermediate- and high-velocity components (vLSR≳ 100km/s) relative to the LMC disc observed in the high- and low-ion absorption profiles. The stellar environments produce strong, narrow (T ≲ 2 x104K) components of Civ and Siiv associated with the LMC disc; in particular they are likely signatures of Hii regions and expanding shells. Broad components are observed in the profiles of Civ, Siiv and Ovi with their widths implying hot, collisionally ionized gas at temperatures of a few times 105K. There is a striking similarity in the Ovi/Civ ratios for the broad LMC and high-velocity components, suggesting much of the material at vLSR≳ 100km/s is associated with the LMC. The velocity of the high-velocity component is large enough to escape altogether the LMC, polluting the intergalactic space between the LMC and the Milky Way. The observed high-ion ratios of the broad LMC and high-velocity components are consistent with those produced in conductive interfaces; such models are also favoured by the apparent kinematically coupling between the high and the weakly ionized species.