  We study the evolution of oxygen abundance radial gradients as a function of
time for the Milky Way Galaxy obtained with our {\sc Mulchem} chemical
evolution model. We review the recent data of abundances for different objects
observed in our Galactic disc. We analyse with our models the role of the
growth of the stellar disc, as well as the effect of infall rate and star
formation prescriptions, or the pre-enrichment of the infall gas, on the time
evolution of the oxygen abundance radial distribution. We compute the radial
gradient of abundances within the {\sl disk}, and its corresponding evolution,
taking into account the disk growth along time. We compare our predictions with
the data compilation, showing a good agreement. Our models predict a very
smooth evolution when the radial gradient is measured within the optical disc
with a slight flattening of the gradient from $\sim -0.057$\,dex\,kpc$^{-1}$ at
$z=4$ until values around $\sim -0.015$\,dex\,kpc$^{-1}$ at $z=1$ and basically
the same gradient until the present, with small differences between models.
Moreover, some models show a steepening at the last times, from $z=1$ until
$z=0$ in agreement with data which give a variation of the gradient in a range
from $-0.02$ to $-0.04$\,de\,kpc$^{-1}$ from $t=10$\,Gyr until now. The
gradient measured as a function of the normalized radius $R/R_{\rm eff}$ is in
good agreement with findings by CALIFA and MUSE, and its evolution with
redshift falls within the error bars of cosmological simulations.
