  Understanding the formation of substructures in protoplanetary disks is vital
for gaining insights into dust growth and the process of planet formation.
Studying these substructures in highly embedded Class 0 objects using the
Atacama Large Millimeter/submillimeter Array (ALMA), however, poses significant
challenges. Nonetheless, it is imperative to do so to unravel the mechanisms
and timing behind the formation of these substructures. In this study, we
present high-resolution ALMA data at Bands 6 and 4 of the NGC1333 IRAS4A Class
0 protobinary system. This system consists of two components, A1 and A2,
separated by 1.8" and located in the Perseus molecular cloud at $\sim$293 pc
distance. To gain a comprehensive understanding of the dust properties and
formation of substructures in the early stages, we conducted a multi-wavelength
analysis of IRAS4A1. Additionally, we sought to address whether the lack of
observed substructures in very young disks, could be attributed to factors such
as high degrees of disk flaring and large scale heights. To explore this
phenomenon, we employed radiative transfer models using RADMC-3D. Our
multi-wavelength analysis of A1 discovered characteristics such as high dust
surface density, substantial dust mass within the disk, and elevated dust
temperatures. These findings suggest the presence of large dust grains compared
to the ones in the interstellar medium (ISM), greater than 100 microns in size
within the region. Furthermore, while there's no direct detection of any
substructure, our models indicate that some, such as a small gap, must be
present. In summary, this result implies that disk substructures may be masked
or obscured by a large scale height in combination with a high degree of
flaring in Class 0 disks. [Abridged]
