We have performed large-scale nucleosynthesis calculations within the high-entropy-wind (HEW) scenario of Type II supernovae. The primary aim was to constrain the conditions for the production of the classical ‘p-only’ isotopes of the light trans-Fe elements. We find, however, that for electron fractions in the range 0.458 ≤ Y_e ≤ 0.478, sizeable abundances of p-, s- and r-process nuclei between ⁶⁴Zn and ⁹⁸Ru are coproduced in the HEW at low entropies (S ≤ 100) by a primary charged-particle process after an α-rich freezeout. With the above Y_e–S correlation, most of the predicted isotopic abundance ratios within a given element, e.g. ⁶⁴Zn(p)/⁷⁰Zn(r) or ⁹²Mo(p)/⁹⁴Mo(p), as well as of neighboring elements, e.g. ⁷⁰Ge(s + p)/⁷⁴Se(p) or ⁷⁴Se(p)/⁷⁸Kr(p) agree with the observed Solar-System ratios. Taking the Mo isotopic chain as a particularly challenging example, we show that our HEW model can account for the production of all 7 stable isotopes, from ‘p-only’ ⁹²Mo, via ‘s-only’ ⁹⁶Mo up to ‘r-only’ ¹⁰⁰Mo. Furthermore, our model is able to reproduce the isotopic composition of Mo in presolar SiC X-grains.