This manuscript represents a spherically symmetric model of a star cluster as a self-gravitating fluid in high curvature gravitational theory. The high curvature terms are used as a mathematical candidate for dark matter in the Star cluster. Different evolutionary phases of star clusters are discussed by using structure scalar techniques along with evolution equations of dynamical terms like isotropic pressure, density homogeneity, homologous, and geodesic behavior. It is concluded that the presence of dark matter directly affects the features of clusters like anisotropic pressure, dissipation, expansion, shear as well as density homogeneity.