Lithium (Li) is a valuable element for testing models of (a) chemical evolution in our Galaxy, (b) stellar interiors, and (c) our early universe when elements first formed. This is because Li is created in a variety of processes in our Galaxy and is also destroyed in the interiors of stars. Studying Li in open star clusters gives us a large sample of depleted Li abundances for different types of stars, but because of the Galactic production of Li, we do not know what Li abundance these star clusters began with. Therefore, we have difficulty evaluating the degree of Li depletion in the cluster stars. In this dissertation I analyze the Li abundances in seven young star clusters and discover that we can measure their initial Li abundance directly. These star clusters also have a range of iron (Fe) abundance, with Fe being the standard tracer of the production of elements, and I find that our initial Li measurements show a positive correlation with Fe abundance. Comparing this Li-Fe correlation to the initial Li abundance of our Sun (from meteoritic data) shows remarkable agreement and suggests that we can apply this correlation to learn the initial Li abundance of older star clusters based on their Fe abundance. This application to older clusters can be used to test models of stellar Li depletion, and the correlation itself can be used directly to test models of Galactic Li production.