The existence of billion-solar-mass quasars at redshifts z ≳ 7 poses a formidable challenge to theories of black hole formation, requiring pathways for the rapid growth of massive seeds. One such pathway may arise from primordial stars powered by dark matter (DM) self-annihilation rather than conventional hydrogen fusion, which could form massive black hole seeds in ordinary cosmological mini-haloes. Here we present a suite of stellar evolution models for DM-powered protostars, computed with the code. We systematically explored a wide parameter space, spanning ambient WIMP densities of ̊ho_̧hi ∼ 10^ GENEC 12 -- 10^ 16 , and gas accretion rates of 10^ -3 -3 -- 10^ -1 ,M_⊙, , to quantify the effects of DM annihilation. A central finding is that for a protostar to grow to supermassive scales (≳ 10^5 , M_⊙), the ambient DM density in the immediate vicinity of the star must exceed a critical threshold of yr^ -1 ̧hi ≳ 5 , 10^ 14 GeV cm ^ -3 . The energy injected by WIMP annihilation inflates the protostar, lowering its surface temperature, which suppresses the ionising feedback that would otherwise halt accretion and significantly delays the onset of hydrogen fusion. This heating also governs the star's final fate; In dense halos (̊ho_̧hi ≳ 10^ 15 , ), stars remain stable against general relativistic instability beyond 10^6 , M_⊙, whereas at lower densities (̊ho_̧hi łesssim 10^ -3 13 , ), they collapse at masses of ∼ 5 : ^ -3 10^5 , M_⊙. Once the DM fuel is exhausted and core burning commences, the protostar contracts and its ionising photon output can reach very high levels ∼ 10^ 53 ̊m s -1 . These distinct evolutionary phases offer clear observational signatures for the , providing a robust, physically grounded pathway for forming heavy black hole seeds in the early Universe. JWST