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[Abridged] We have studied the optical spectra of 28 O- and early B-typestars in the Large Magellanic Cloud, 22 of which are associated with the youngstar-forming region N11. Stellar parameters are determined using an automatedfitting method, combining the stellar atmosphere code FASTWIND with thegenetic-algorithm optimisation routine PIKAIA. Results for stars in the LH9 andLH10 associations of N11 are consistent with a sequential star formationscenario, in which activity in LH9 triggered the formation of LH10. Our samplecontains four stars of spectral type O2, of which the hottest is found to be~49-54 kK (cf. ~45-46 kK for O3 stars). The masses of helium-enriched dwarfsand giants are systematically lower than those implied by non-rotatingevolutionary tracks. We interpret this as evidence for efficientrotationally-enhanced mixing, leading to the surfacing of primary helium and toan increase of the stellar luminosity. This result is consistent with findingsfor SMC stars by Mokiem et al. For bright giants and supergiants no suchmass-discrepancy is found, implying that these stars follow tracks of modestly(or non-)rotating objects. Stellar mass-loss properties were found to beintermediate to those found in massive stars in the Galaxy and the SMC, andcomparisons with theoretical predictions at LMC metallicity yielded goodagreement over the luminosity range of our targets, i.e. 5.0 < log L/L(sun) <6.1.

The VLT-FLAMES survey of massive stars: Wind properties and evolution of hot massive stars in the LMC