We present our results on measurements of the neutral hydrogen (HI) mass fraction in galaxy cluster environment of a nearby cluster Abell 262 (A262), and investigate the possible physical processes that lead to our estimation of HI mass fraction in this cluster. We conduct a spectroscopic analysis to define a true cluster membership around Abell radius of the cluster, from which we estimate the virial mass of the whole cluster based on the velocity dispersion analysis, and later use data from a 21-cm single-pointing observation to deduce the global HI mass fraction in the cluster. It is found that the HI mass, MHI, and HI mass fraction, FHI, of A262 are equal to be about (4.33±0.32)×1011M☉ and (1.01±0.09)×10-3, respectively, in which the latter agrees with previous findings. We have also shown that the fraction of stellar mass in A262 is about (8.25±0.14)×10-3, and falls within the range of the widely accepted value. We discuss several physical mechanisms that contribute to the derived HI mass fraction of A262. We also emphasize that the FHI can be used as a proxy of efficiency of physical processes in clusters, if we have a large sample of galaxy clusters with available HI data.