  We present the integrated VLT-MUSE spectrum of the central 2'x2' (30x30
pc$^{2}$) of NGC 2070, the dominant giant HII region of the Tarantula Nebula in
the Large Magellanic Cloud, together withan empirical far-ultraviolet spectrum
constructed via LMC template stars from the ULLYSES survey and Hubble Tarantula
Treasury Project UV photometry. NGC 2070 provides a unique opportunity to
compare results from individual stellar populations (e.g. VLT FLAMES Tarantula
Survey) in a metal-poor starburst region to the integrated results from the
population synthesis tools Starburst99, Charlot & Bruzual and BPASS. The
metallicity of NGC 2070 inferred from standard nebular strong line calibrations
is 0.4$\pm$0.1 dex lower than obtained from direct methods. The Halpha inferred
age of 4.2 Myr from Starburst99 is close to the median age of OB stars within
the region, although individual stars span a broad range of 1-7 Myr. The
inferred stellar mass is close to that obtained for the rich star cluster R136
within NGC 2070, although this contributes only 21% to the integrated far-UV
continuum. HeII 1640 emission is dominated by classical WR stars and main
sequence WNh+Of/WN stars. 18% of the NGC~2070 far UV continuum flux arises from
very massive stars with >100 Msun, including several very luminous Of
supergiants. None of the predicted population synthesis models at low
metallicities are able to successfully reproduce the far-UV spectrum of NGC
2070. We attribute issues to the treatment of mass-loss in very massive stars,
the lack of contemporary empirical metal-poor templates, plus WR stars produced
via binary evolution.
