  We present an extended grid of state-of-the art stellar models for low-mass
stars including updated physics (nuclear reaction rates, surface boundary
condition, mass-loss rate, angular momentum transport, torque and
rotation-induced mixing prescriptions).
  We aim at evaluating the impact of wind braking, realistic atmospheric
treatment, rotation and rotation-induced mixing on the structural and
rotational evolution from the pre-main sequence to the turn-off.
  Using the STAREVOL code, we provide an updated PMS grid. We compute stellar
models for 7 different metallicities, from [Fe/H] = -1 dex to [Fe/H] = +0.3 dex
with a solar composition corresponding to $Z=0.0134$. The initial stellar mass
ranges from 0.2 to 1.5\Ms with extra grid refinement around one solar mass. We
also provide rotating models for three different initial rotation rates (slow,
median and fast) with prescriptions for the wind braking and disc-coupling
timescale calibrated on observed properties of young open clusters. The
rotational mixing includes an up-to-date description of the turbulence
anisotropy in stably stratified regions.
  The overall behaviour of our models at solar metallicity -- and its
constitutive physics -- is validated through a detailed comparison with a
variety of distributed evolutionary tracks. The main differences arise from the
choice of surface boundary conditions and initial solar composition.
  The models including rotation with our prescription for angular momentum
extraction and self-consistent formalism for angular momentum transport are
able to reproduce the rotation period distribution observed in young open
clusters over a broad mass-range.
  These models are publicly available and may be used to analyse data coming
from present and forthcoming asteroseismic and spectroscopic surveys such as
Gaia, TESS and PLATO.
