The existence of temperate giant planets like Jupiter has been previously linked to the development of gaps in the protoplanetary disk (e.g. by photoevaporation) and trapping of critial Stokes number particles ("pebbles) at an accompanying pressure maximum (van der Marel & Mulders 2021). Also, interior magnetothermal winds from the disk could block EUV and soft X-rays from reaching the disk further out, driving photoevaporation (Pascucci et al. 2020). Gaidos et al. (2025) proposed that the presence or absence of inner disk winds govern the lifetime and structure evolution around single low-mass stars in low UV environments, and that the apperance of inner disk winds, in turn, are regulated by the evolving positions of the co-rotation and disk truncation radius. Here, in an ensemble approach, we combine this model of disk evolution with a parametric model of pebble drift and a crition for runaway gas accretion to predict the formation and location of temperate giant planets. We compare predicted and observed orbital distributions and trends of occurrence with stellar mass and metallicity, and consider the sensitivity to pebble drift rate and critical core mass.