The Gemini Planet Imager (GPI) is a high contrast imaging instrument designed to directly detect and characterize young Jupiter-mass exoplanets. After six years of operation at Gemini South in Chile, the instrument is being upgraded and moved to Gemini North in Hawaii as GPI 2.0. As part of this upgrade, several improvements will be made to the adaptive optics (AO) system. This includes replacing the current Shack-Hartmann wavefront sensor (WFS) with a pyramid wavefront sensor (PWFS) and a custom EMCCD. These changes are expected to increase GPI's sky coverage by accessing fainter targets, improving corrections on fainter stars and allowing faster and ultra-low latency operations on brighter targets. The PWFS subsystem is being independently built and tested to verify its performance before its integration into the GPI 2.0 instrument. In this paper, we will present the design and pre-integration test plan of the PWFS.