  Measurements of the cluster abundance as a function of mass and redshift
provide an important cosmological test that probe not only the expansion rate
but also the growth of perturbations. In this paper we adopt a scalar field
scenario which admits both thawing and freezing solutions from an appropriate
choice of the model parameters and derived all relevant expressions to
calculate the mass function and the cluster number density. We discuss the
ability of cluster observations to distinguish between these scalar field
behaviors and the standard $\Lambda$CDM scenario by considering the eROSITA and
SPT cluster surveys.
