Context : Our understanding of the formation and early evolution of globular clusters ( GCs ) has been totally overthrown with the discovery of the peculiar chemical properties of their long-lived host stars .

Aims : As a consequence , the interpretation of the observed color-magnitude diagrams and of the properties of the GC stellar populations requires the use of stellar models computed with relevant chemical compositions .

Methods : We present a grid of 224 stellar evolution models for low-mass stars with initial masses between 0.3 and 1.0 M _ { \odot } and initial helium mass fraction between 0.248 and 0.8 computed for [ Fe/H ] =-1.75 with the stellar evolution code STAREVOL .
This grid is made available to the community .

Results : We explore the implications of the assumed initial chemical distribution for the main properties of the stellar models : evolution paths in the Hertzsprung-Russel diagram ( HRD ) , duration and characteristics of the main evolutionary phases , and the chemical nature of the white dwarf remnants .
We also provide the ranges in initial stellar mass and helium content of the stars that populate the different regions of the HRD at the ages of 10 and 13.4 Gyr , which are typical for Galactic GCs .

Conclusions :