The Sloan Digital Sky Survey (SDSS) has constructed a large-format mosaic CCD camera for its photometric survey. The camera consists of two arrays: a photometric array with 30 2048×2048 SITe/Tektronix CCDs (24 micron pixels) and an astrometric array with 24 400×2048 CCDs. The photometric array will perform photometry in five color bands, while the astrometric array will tie bright standard stars to the objects imaged in the photometric camera. The camera is designed to achieve high astrometric accuracy, with a limiting magnitude of about 22.1 mag for the $u'$ band and 23.2 mag for the $g'$ band. The optical design of the camera includes a modified Ritchey-Chrétien telescope with two aspheric corrector lenses to minimize distortion and achieve a nearly flat focal surface. The camera's performance is characterized by its efficiency, which is 4.8 m²deg², allowing for deeper surveys and simultaneous imaging in five color bands. The camera's design and construction address challenges such as housing large arrays of CCDs, achieving high astrometric accuracy, and managing complex electronic systems. The paper provides detailed engineering and technical details of the camera, including the optical design, CCD characteristics, mechanical design, and electronic systems.The Sloan Digital Sky Survey (SDSS) has constructed a large-format mosaic CCD camera for its photometric survey. The camera consists of two arrays: a photometric array with 30 2048×2048 SITe/Tektronix CCDs (24 micron pixels) and an astrometric array with 24 400×2048 CCDs. The photometric array will perform photometry in five color bands, while the astrometric array will tie bright standard stars to the objects imaged in the photometric camera. The camera is designed to achieve high astrometric accuracy, with a limiting magnitude of about 22.1 mag for the $u'$ band and 23.2 mag for the $g'$ band. The optical design of the camera includes a modified Ritchey-Chrétien telescope with two aspheric corrector lenses to minimize distortion and achieve a nearly flat focal surface. The camera's performance is characterized by its efficiency, which is 4.8 m²deg², allowing for deeper surveys and simultaneous imaging in five color bands. The camera's design and construction address challenges such as housing large arrays of CCDs, achieving high astrometric accuracy, and managing complex electronic systems. The paper provides detailed engineering and technical details of the camera, including the optical design, CCD characteristics, mechanical design, and electronic systems.