The star formation history of the universe reveals that galaxies most actively build their stellar mass at cosmic noon, roughly 10 billion years ago, with a decrease toward present-day. The resulting metal-enriched material ejected from these galaxies due to supernovae and stellar feedback is deposited into the circumgalactic medium (CGM), which is a massive reservoir of diffuse, multiphase gas out to radii of $∼200$ kpc. The CGM is the interface between the intergalactic medium and the galaxy, through which accreting filaments of near-pristine gas must pass to contribute new star formation material to the galaxy, and outflowing gas is later recycled. Simulating these baryon cycle flows is crucial for accurately modelling galaxy evolution. We examine these multiphase CGM gas flows with the quasar absorption line technique, primarily focusing on the low-ionization MgII absorption doublet (T$∼10^{4}$ K), with additional multiphase ions such as Lyman alpha, FeII, and CIV. With the combination of HST images, high-resolution UVES/VLT quasar spectra, and cutting-edge IFU data from the Keck Cosmic Web Imager, we quantify the gas kinematics and metallicities of outflowing gas at 69 kpc along the minor axis of an edge-on ($i=85^{∘}$) galaxy at cosmic noon ($z_{\rm gal}=2.070$). Connecting these results to our Multiphase Galaxy Halos Survey at $z∼0.3$, we study the evolution of CGM kinematics and metallicities over nearly 10 billion years.