  Evolution and abundance of the large-scale structures we observe today, such
as clusters of galaxies, is sensitive to the statistical properties of dark
matter primordial density fluctuations, which is assumed to follow a Gaussian
probability distribution function. Within this assumption, a significant
disagreement have been found between clusters counts made by Planck and their
prediction when calibrated by CMB angular power spectrum. The purpose of this
work is to relax the Gaussianty assumption and test if Non-Gaussianity in dark
matter primordial density fluctuations, could alleviate the tension.
