The past 25 years have seen the development of a collection of star formation rate (SFR) indicators in galaxies, covering the electromagnetic spectrum from X-rays to the radio. Nearly all of them suffer severe systematic errors, which arise from the highly variable amounts and opacities of interstellar dust in galaxies. The advent of comprehensive multi-wavelength surveys of galaxies such as the Spitzer SINGS and LVL legacy projects now make it possible to calibrate quasi-bolometric SFR indices that combine observations of the unobscured star formation in the visible or UV with the emission of the dust-obscured star formation in the infrared or radio. The best of these reduce the level of random and systematic uncertainties in individual SFRs from factors of a few (for single wavelength indices) to the 10-20% level, at which point dust no longer is the dominant error source. This talk will present a progress report on our efforts to construct a complete multi-wavelength "toolbox" of SFR measures, which can be applied in nearby and distant galaxy samples alike.