The Atacama Large Millimeter/Submillimeter Array (ALMA), an interferometric radio telescope will have 66 array elements when complete. The ALMA Front End is designed to accommodate up to 10 receiver bands covering most of the wavelength range from 10 to 0.3 mm. Superconductor-insulator-superconductor (SIS) mixers are employed for Bands 3 (similar to 3 mm) through 10 (similar to 0.3 mm). Ordinarily the SIS bias is selected to achieve the lowest receiver noise temperatures. However, in order to obtain the lowest detection threshold, the SIS bias also needs to be optimized with respect to receiver stability. There are also other parameters to be optimized such as the magnetic field strength used to suppress the Josephson currents and avoidance of Shapiro. This paper will summarize the results of work carried out to derive the optimal operating parameters for the large number of mixers in use on the telescope so as to keep the telescope operating reliably and repeatably.