The observations of high-redshifts quasars at z greater than or similar to 6 have revealed that supermassive black holes (SMBHs) of mass were already in place within the first similar to Gyr after the big bang. Supermassive stars (SMSs) with masses are potential seeds for these observed SMBHs. A possible formation channel of these SMSs is the interplay of gas accretion and runaway stellar collisions inside dense nuclear star clusters (NSCs). However, mass-loss due to stellar winds could be an important limitation for the formation of the SMSs and affect the final mass. In this paper, we study the effect of mass-loss driven by stellar winds on the formation and evolution of SMSs in dense NSCs using idealized N-body simulations. Considering different accretion scenarios, we have studied the effect of the mass-loss rates over a wide range of metallicities Z(*) = [.001-1]Z(circle dot) and Eddington factors . For a high accretion rate of , SMSs with masses could be formed even in a high metallicity environment. For a lower accretion rate of , SMSs of masses can be formed for all adopted values of Z(*) and f(Edd), except for Z(*) = Z(circle dot) and f(Edd) = 0.7 or 0.9. For Eddington accretion, SMSs of masses can be formed in low metallicity environments with Z(*) less than or similar to 0.01Z(circle dot). The most massive SMSs of masses can be formed for Bondi-Hoyle accretion in environments with Z(*) less than or similar to 0.5Z(circle dot). An intermediate regime is likely to exist where the mass-loss from the winds might no longer be relevant, while the kinetic energy deposition from the wind could still inhibit the formation of a very massive object.