  We present a spatially resolved stellar population study of the inner
$\sim$200\,pc radius of NGC4303 based on near-infrared integral field
spectroscopy with SINFONI/VLT at a spatial resolution of 40-80pc and using the
STARLIGHT code. We found the distribution of the stellar populations presents a
spatial variation, suggesting an age stratification. Three main structures
stand out. Two nuclear blobs, one composed by young stars (t $\leq$ 50Myr) and
one with intermediate-age stars (50Myr $<$ t $\leq$ 2Gyr) both shifted from the
centre. The third one is an internal intermediate-age spiral arm-like
structure, surrounding the blob of young stars. Our results indicate star
formation has occurred through multiple bursts in this source. Furthermore, the
youngest stellar populations (t $\lesssim$ 2Gyr) are distributed along a
circumnuclear star-forming ring with r$\sim$250pc. The ring displays star
formation rates (SFRs) in the range of 0.002-0.14M$_{\odot}$yr$^{-1}$, favoring
the `pearls-on-a-string' scenario. The old underlying bulge stellar population
component (t $>$ 2Gyr) is distributed outside the two blob structures. For the
nuclear region (inner $\sim$60pc radius) we derived a SFR of
0.43\,M$_{\odot}$yr$^{-1}$ and found no signatures of non-thermal featureless
continuum and hot dust emission, supporting the scenario in which a
LLAGN/LINER-like source is hidden in the centre of NGC4303. Thus, our results
reveal a rather complex star formation history in NGC4303, with different
stellar population components coexisting with a low efficiency accreting black
hole in its centre.
