  The G305 HII complex (G305.4+0.1) is one of the most massive star forming
structures yet identified within the Galaxy. It is host to many massive stars
at all stages of formation and evolution, from embedded molecular cores to post
main-sequence stars. Here, we present a detailed near-infrared analysis of the
two central star clusters Danks 1 and Danks 2, using HST+NICMOS imaging and
VLT+ISAAC spectroscopy. We find that the spectro-photometric distance to the
clusters is consistent with the kinematic distance to the G305 complex, an
average of all measurements giving a distance of 3.8\pm0.6kpc. From analysis of
the stellar populations and the pre-main-sequence stars we find that Danks 2 is
the elder of the two clusters, with an age of 3^{+3}_{-1}Myr. Danks 1 is
clearly younger with an age of 1.5^{+1.5}_{-0.5}Myr, and is dominated by three
very luminous H-rich Wolf-Rayet stars which may have masses \geq100\msun. The
two clusters have mass functions consistent with the Salpeter slope, and total
cluster masses of 8000\pm1500\msun\ and 3000\pm800\msun\ for Danks 1 and Danks
2 respectively. Danks 1 is significantly the more compact cluster of the two,
and is one of the densest clusters in the Galaxy with $\log (\rho/M_{\odot}{\rm
pc}^{-3}) = 5.5^{+0.5}_{-0.4}$. In addition to the clusters, there is a
population of apparently isolated Wolf-Rayet stars within the molecular cloud's
cavity. Our results suggest that the star-forming history of G305 began with
the formation of Danks 2, and subsequently Danks 1, with the origin of the
diffuse evolved population currently uncertain. Together, the massive stars at
the centre of the G305 region appear to be clearing away what is left of the
natal cloud, triggering a further generation of star formation at the cloud's
periphery.
