The article presents positional, structural, and dynamical parameters for all dwarf galaxies in and around the Local Group, with over 100 galaxies identified within 3 Mpc of the Sun. These galaxies span a range of environments, from satellite systems of the Milky Way (MW) and Andromeda (M31) to isolated dwarfs in the Local Group's outer regions. The study discusses the observational understanding of this sample, including distance, velocity, magnitude, metallicity, and structural characteristics. Tables are provided for continuous updates as observational capabilities improve. The article explores the membership and spatial extent of the MW and M31 sub-groups, the morphological diversity of the sample, and time-scales for Local Group members. Scaling relations and mean stellar metallicity trends are presented, along with the possible origin of a "floor" in central surface brightness at faint magnitudes. The study highlights the importance of the Local Group in understanding dwarf galaxy formation and evolution. It discusses the selection criteria for the sample, including resolved stellar populations, and the exclusion of galaxies with uncertain distances. The article also addresses the challenges of studying dwarf galaxies, such as the influence of environmental factors and the limitations of observational data. It emphasizes the need for future surveys to improve the census of Local Group galaxies and their neighbors. The study concludes that the Local Group provides a unique laboratory for studying dwarf galaxy properties, with ongoing research expected to refine our understanding of their formation and evolution.The article presents positional, structural, and dynamical parameters for all dwarf galaxies in and around the Local Group, with over 100 galaxies identified within 3 Mpc of the Sun. These galaxies span a range of environments, from satellite systems of the Milky Way (MW) and Andromeda (M31) to isolated dwarfs in the Local Group's outer regions. The study discusses the observational understanding of this sample, including distance, velocity, magnitude, metallicity, and structural characteristics. Tables are provided for continuous updates as observational capabilities improve. The article explores the membership and spatial extent of the MW and M31 sub-groups, the morphological diversity of the sample, and time-scales for Local Group members. Scaling relations and mean stellar metallicity trends are presented, along with the possible origin of a "floor" in central surface brightness at faint magnitudes. The study highlights the importance of the Local Group in understanding dwarf galaxy formation and evolution. It discusses the selection criteria for the sample, including resolved stellar populations, and the exclusion of galaxies with uncertain distances. The article also addresses the challenges of studying dwarf galaxies, such as the influence of environmental factors and the limitations of observational data. It emphasizes the need for future surveys to improve the census of Local Group galaxies and their neighbors. The study concludes that the Local Group provides a unique laboratory for studying dwarf galaxy properties, with ongoing research expected to refine our understanding of their formation and evolution.