Most young, low-mass stars are surrounded by accretion disks. The increasing number of planets detected around main-sequence stars strongly suggests that planets will form in many, if not all, disks. A broad goal is to connect the properties and evolution of disks with the formation and diversity of planetary systems. Millimeter-wavelength interferometric observations play a central role in these studies by probing the bulk of the gas and dust in disks. In this talk, I present recent results to measure the structure, grain growth, and temporal evolution of disks with an emphasis on ALMA, CARMA, and VLA observations. I will also highlight future directions with ALMA.