Grids of stellar models with rotation VII: Models from 0.8 to 300
  M$_\odot$ at super-solar metallicity (Z = 0.020)
  We present a grid of stellar models at super-solar metallicity (Z = 0.020)
extending the previous grids of Geneva models at solar and sub-solar
metallicities. A metallicity of Z = 0.020 was chosen to match that of the inner
Galactic disk. A modest increase of 43% (=0.02/0.014) in metallicity compared
to solar models means that the models evolve similarly to solar models but with
slightly larger mass loss. Mass loss limits the final total masses of the
super-solar models to 35 M$_\odot$ even for stars with initial masses much
larger than 100 M$_\odot$. Mass loss is strong enough in stars above 20
M$_\odot$ for rotating stars (25 M$_\odot$ for non-rotating stars) to remove
the entire hydrogen-rich envelope. Our models thus predict SNII below 20
M$_\odot$ for rotating stars (25 M$_\odot$ for non-rotating stars) and SNIb
(possibly SNIc) above that. We computed both isochrones and synthetic clusters
to compare our super-solar models to the Westerlund 1 (Wd1) massive young
cluster. A synthetic cluster combining rotating and non-rotating models with an
age spread between log10 (age/yr) = 6.7 and 7.0 is able to reproduce
qualitatively the observed populations of WR, RSG and YSG stars in Wd1, in
particular their simultaneous presence at log10(L/L$_\odot$) = 5-5.5. The
quantitative agreement is imperfect and we discuss the likely causes: synthetic
cluster parameters, binary interactions, mass loss and their related
uncertainties. In particular, mass loss in the cool part of the HRD plays a key
role.
