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Most of what we know about the formation of stars, and essentially everythingwe know about the formation of planets, comes from observations of our solarneighborhood within 2 kpc of the Sun. Before 2018, accurate distancemeasurements needed to turn the 2D Sky into a faithful 3D physical picture ofthe distribution of stars, and the interstellar matter that forms them, werefew and far between. Here, we offer a holistic review of how, since 2018, datafrom the Gaia mission are revealing previously unseen and often unexpected 3Ddistributions of gas, dust, and young stars in the solar neighborhood. Wesummarize how new extinction-based techniques yield 3D dust maps and how thedensity structure mapped out offers key context for measuring young stars' 3Dpositions from Gaia and VLBI. We discuss how a subset of young stars in Gaiawith measured radial velocities and proper motions is being used to recover 3Dcloud motion and characterize the internal dynamics of individual star-formingregions. We review relationships between newly-identified clusters and streamsof young stars and the molecular interstellar medium from which they evolve.The combination of these measures of gas and stars' 3D distribution and 3Dmotions provides unprecedented data for comparison with simulations andreframes our understanding of local star formation in a larger Galacticcontext. This new 3D view of our solar neighborhood in the age of Gaia showsthat star-forming regions once thought to be isolated are often connected onkiloparsec scales, causing us to reconsider models for the arrangement of gasand young stars in galaxies.

The Solar Neighborhood in the Age of Gaia